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GSC 03089-00929

Coordinates: Sky map 17h 52m 07s, +37° 32′ 46″
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GSC 03089-00929 / Pipoltr

A light curve for V1434 Herculis, plotted from TESS data,[1] the 1.306 day interval between planet transits is shown in red.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Hercules
Right ascension 17h 52m 07.0184s[2]
Declination +37° 32′ 46.237″[2]
Apparent magnitude (V) 12.4
Characteristics
Spectral type G
Apparent magnitude (B) 13.114 ±0.009[3]
Apparent magnitude (V) 12.402 ±0.006[3]
Apparent magnitude (I) 11.603000 ±0.010[3]
Apparent magnitude (J) 11.015 ±0.022[3]
Apparent magnitude (H) 10.655000 ±0.030[3]
Apparent magnitude (K) 10.608000 ±0.028[3]
Variable type planetary transits[3][4]
Astrometry
Proper motion (μ) RA: −24.462(10) mas/yr[2]
Dec.: 34.772(11) mas/yr[2]
Parallax (π)4.3106 ± 0.0091 mas[2]
Distance757 ± 2 ly
(232.0 ± 0.5 pc)
Absolute magnitude (MV)5.39±0.11[5]
Details
Mass0.928+0.028
−0.048[5] M☉
Radius0.826±0.012[6] R☉
Luminosity0.625+0.066
−0.058[5] L☉
Surface gravity (log g)4.57±0.01[6] cgs
Temperature5650±75[5] K
Metallicity [Fe/H]−0.19±0.08[5] dex
Rotational velocity (v sin i)1.5±1.0 km/s
Age0.9+2.8
−0.8[5] Gyr
Other designations
TrES-3 Parent Star, 1SWASP J175207.01+373246.3, UCAC2 45017453,[3] V1434 Her
Database references
SIMBADdata

GSC 03089-00929 is a magnitude 12 star located approximately 757 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun.[3] This star is identified in SIMBAD as a variable star per the 1SWASP survey.[7]

The star GSC 03089-00929 is named Pipoltr. The name was selected in the NameExoWorlds campaign by Liechtenstein, during the 100th anniversary of the IAU. In the local dialect of Triesenberg, Pipoltr is a bright and visible butterfly.[8][9]

Planetary system

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In 2007 the TrES program found exoplanet TrES-3b, later named Umbäässa, orbiting this star by using the transit method.[10]

The transit timing variation analysis did not reveal any additional planets in the system as of 2020,[11] and the physical mechanism underlying transit timing variations remains unexplained as in 2022.[12]

The GSC 03089-00929 planetary system[13][6][5]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
TrES-3b / Umbäässa 1.910+0.075
−0.080 MJ 		0.02282+0.00023
−0.00040 		1.30618652(4) 0 (fixed) 81.89±0.12° 1.381±0.033 RJ

See also

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References

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  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 27 August 2024.
  2. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c d e f g h i "NAME TrES-3 Parent Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-23.
  4. ^ Lister, T. A.; West, R. G.; Wilson, D. M.; Collier Cameron, A.; Clarkson, W. I.; Street, R. A.; Enoch, B.; Parley, N. R.; et al. (June 30, 2007). "SuperWASP-North extrasolar planet candidates: candidates from fields 17h<RA<18h" (PDF). Monthly Notices of the Royal Astronomical Society. 379 (2): 647–662. arXiv:0705.2603. Bibcode:2007MNRAS.379..647L. doi:10.1111/j.1365-2966.2007.11948.x. S2CID 14333676.
  5. ^ a b c d e f g Sozzetti, Alessandro; et al. (2009). "A New Spectroscopic and Photometric Analysis of the Transiting Planet Systems TrES-3 and TrES-4". The Astrophysical Journal. 691 (2): 1145–1158. arXiv:0809.4589. Bibcode:2009ApJ...691.1145S. doi:10.1088/0004-637X/691/2/1145. S2CID 3741198.
  6. ^ a b c Püsküllü, Ç.; et al. (2017). "Photometric investigation of hot exoplanets: TrES-3b and Qatar-1b". New Astronomy. 55: 39–47. arXiv:1704.03697. Bibcode:2017NewA...55...39P. doi:10.1016/j.newast.2017.04.001. S2CID 119208251.
  7. ^ "Objects in reference 2007MNRAS.379..647L". Centre de Données astronomiques de Strasbourg. Retrieved 2009-05-03.
  8. ^ "Approved names". NameExoworlds. Archived from the original on 2019-12-19. Retrieved 2020-01-02.
  9. ^ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  10. ^ O'Donovan, Francis T.; Charbonneau, David; Bakos, Gáspár Á.; Mandushev, Georgi; Dunham, Edward W.; Brown, Timothy M.; Latham, David W.; Torres, Guillermo; et al. (July 1, 2007). "TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31-Hour Orbit". Astrophysical Journal Letters. 663 (1): L37–L40. arXiv:0705.2004. Bibcode:2007ApJ...663L..37O. doi:10.1086/519793. S2CID 17637874.
  11. ^ Mannaday, Vineet Kumar; Thakur, Parijat; Jiang, Ing-Guey; Sahu, D. K.; Joshi, Y. C.; Pandey, A. K.; Joshi, Santosh; Yadav, Ram Kesh; Su, Li-Hsin; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey; Moskvin, Vasilii; Ignatov, Vladimir; Vaňko, M.; Püsküllü, Ç. (2020). "Probing Transit Timing Variation and Its Possible Origin with 12 New Transits of TrES-3b". The Astronomical Journal. 160 (1): 47. arXiv:2006.00599. Bibcode:2020AJ....160...47M. doi:10.3847/1538-3881/ab9818. S2CID 219176648.
  12. ^ Mannaday, Vineet Kumar; Thakur, Parijat; Southworth, John; Jiang, Ing-Guey; Sahu, D. K.; Mancini, L.; Vaňko, M.; Kundra, Emil; Gajdoš, Pavol; a-Thano, Napaporn; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey (2022), "Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data", The Astronomical Journal, 164 (5): 198, arXiv:2209.04080, Bibcode:2022AJ....164..198M, doi:10.3847/1538-3881/ac91c2, S2CID 252185524
  13. ^ MacKebrandt, F.; et al. (2017). "Transmission spectroscopy of the hot Jupiter TrES-3 b: Disproof of an overly large Rayleigh-like feature". Astronomy and Astrophysics. 608. A26. arXiv:1709.06124. Bibcode:2017A&A...608A..26M. doi:10.1051/0004-6361/201730512. S2CID 53995250.
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